Authors: Sylwester Kornowski
It is assumed in the mainstream cosmology that at the Chandrasekhar limit the white dwarfs explode due to the conditions in a Fermi gas. Here, within the Scale-Symmetric Theory (SST), we showed that there appears the tower of the Chandrasekhar limits and that the stars/white-dwarfs with the threshold masses explode via a neutron-star state. Neutron stars behave as liquid crystal. There are the needed flat structures and the elongated rectangular prisms. There appears the upper limit for mass of neutron star, i.e. of the neutron black hole, equal to 24.81 solar masses. But due to perfect energy flow from core of a star toward its surface there as well appear at least three Chandrasekhar limits i.e. masses of stars which explode as Type Ia supernovae via sudden collapse of whole star to the neutron-star state which leads to violent full volumetric explosion so there is not created a neutron-star remnant – the threshold masses are 1.395, 11.20 and 0.891 solar masses. The first mass is the very well known Chandrasekhar limit whereas the second was the mass of, for example, the SN 1987A supernova. Energy is carried by the condensates of the Einstein-spacetime components that are the black holes in respect of the weak interactions or is carried by energetic neutrinos. The condensates with a mass of 52.828 MeV are produced in centres of muons, with a mass of 424.124 MeV are produced in centres of baryons, whereas the characteristic energy of neutrinos is the one fourth of the mass of neutral pion (33.743 MeV). Their number densities increase rapidly for the threshold masses of stars. Here, as well, are calculated the lower (0.000768 s) and upper (4,228 s) limits for spin periods of pulsars i.e. for stars with neutron core and iron crust. Presented here model is very simple and leads to observational facts.
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